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Radio-loud quasars (RLQs) are more X-ray luminous than predicted by theX-ray-optical/UV relation (i.e. $L_\mathrm{x}\propto L_\mathrm{uv}^\gamma$) forradio-quiet quasars (RQQs). The excess X-ray emission depends on theradio-loudness parameter ($R$) and radio spectral slope ($\alpha_\mathrm{r}$).We construct a uniform sample of 729 optically selected RLQs with highfractions of X-ray detections and $\alpha_\mathrm{r}$ measurements.We find thatsteep-spectrum radio quasars (SSRQs; $\alpha_\mathrm{r}\le-0.5$) follow aquantitatively similar $L_\mathrm{x}\propto L_\mathrm{uv}^\gamma$ relation asthat for RQQs, suggesting a common coronal origin for the X-ray emission ofboth SSRQs and RQQs. However, the corresponding intercept of SSRQs is largerthan that for RQQs and increases with $R$, suggesting a connection between theradio jets and the configuration of the accretion flow. Flat-spectrum radioquasars (FSRQs; $\alpha_\mathrm{r}>-0.5$) are generally more X-ray luminousthan SSRQs at given $L_\mathrm{uv}$ and $R$, likely involving more physicalprocesses. The emergent picture is different from that commonly assumed wherethe excess X-ray emission of RLQs is attributed to the jets. We thus performmodel selection to comparecritically these different interpretations, whichprefers the coronal scenario with a corona-jet connection. A distinct jetcomponent is likely important for only a small portion of FSRQs.The corona-jet,disk-corona, and disk-jet connections of RLQs are likely driven by independentphysical processes. Furthermore, the corona-jet connection implies thatsmall-scale processesin the vicinity of SMBHs, probably associated with themagnetic flux/topology instead of black-hole spin, are controlling theradio-loudness of quasars.

The $L_\mathrm{x}$-$L_\mathrm{uv}$-$L_\mathrm{radio}$ relation and corona-disk-jet connection in optically selected radio-loud quasars